DOCSLIB.ORG

Physics and Astrophysics

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Physics and Astrophysics NewsNews fromfrom thethe NSFNSF DivisionDivision ofof PhysicsPhysics JoeJoe DehmerDehmer DivisionDivision ofof PhysicsPhysics BPABPA NovemberNovember 6,6, 20092009 Division of Physics AMOP Theoretical Gravitational Physics Physics Physics Elementary Nuclear Education & Particle Physics Physics Interdisc. Res. Part. & Nucl. Physics of Accelerator Phy. Astrophysics Living Systems & Phy. Instrum. Physics Physics @ Front.Centers Inform. Front. PHYSICSPHYSICS** FRONTIERSFRONTIERS,, circacirca 20092009 •• BoseBose--EinsteinEinstein Condensates,Condensates, AtomAtom ““LasersLasers”” •• DarkDark Matter,Matter, DarkDark EnergyEnergy,, CosmologyCosmology •• GravitationalGravitational WavesWaves (GW),(GW), GWGW AstronomyAstronomy •• NewNew FundamentalFundamental ParticlesParticles andand LawsLaws >> TeVTeV •• νν physicsphysics andand astrophysicsastrophysics •• StringString Theory,Theory, BranesBranes,, Duality,Duality, QuantumQuantum GravityGravity •• QuarkQuark--GluonGluon Plasma,Plasma, SupernovaSupernova DynamicsDynamics •• UltraUltra--Fast,Fast, UltraUltra--IntenseIntense LaserLaser FieldsFields •• CyberscienceCyberscience,, QuantumQuantum InformationInformation ScienceScience •• BiophysicsBiophysics ofof SingleSingle Molecules,Molecules, Cells,Cells, NetworksNetworks •• Complexity,Complexity, EmergentEmergent BehaviorBehavior * CMP in Division of Materials Research * CMP in Division of Materials Research 3 BROAD,BROAD, COMMUNITYCOMMUNITY--BASEDBASED ADVICEADVICE •• AdAd HocHoc andand PanelPanel ReviewsReviews •• CommitteeCommittee ofof VisitorsVisitors •• HighHigh EnergyEnergy PhysicsPhysics AdvisoryAdvisory PanelPanel •• NuclearNuclear ScienceScience AdvisoryAdvisory CommitteeCommittee •• AstronomyAstronomy andand AstrophysicsAstrophysics AdvisoryAdvisory CommitteeCommittee •• MathematicalMathematical andand PhysicalPhysical SciencesSciences AdvisoryAdvisory CommitteeCommittee •• AmericanAmerican PhysicalPhysical SocietySociety DivisionsDivisions •• NationalNational ResearchResearch CouncilCouncil CommitteesCommittees •• NationalNational ScienceScience andand TechnologyTechnology CouncilCouncil WorkingWorking GroupsGroups •• WorkshopsWorkshops 4 AnAn ExampleExample ofof EmergenceEmergence ofof NewNew DiscoveryDiscovery PotentialPotential • What is dark matter? • What is dark energy? • How did the universe begin? • Was Einstein right about gravity? • How have ν shaped the universe? • What are nature’s most energetic particles? • Are protons stable? • Are there new states of matter at exceedingly high density/energy? • Are there additional dimensions? • How were elements Fe to U made? • Is a new theory needed at the highest energies and EM Fields? 5 AstroparticleAstroparticle PhysicsPhysics ProjectsProjects • Gravitational Waves: LIGO/AdvLIGO (GEO, VIRGO, TAMA, 11 countries) • Cosmological Neutrinos: IceCube (NSF-OPP, Germany, Sweden, Belgium) • Underground Physics: DUSEL (DOE-HEP, NP) • Dark Matter: CDMS, XENON, WARP, ZEPLIN, LUX, DRIFT, COUPP (NSF-AST, DOE-HEP, INFN, PPARC, Germany, Poland) • Cosmic Rays: AUGER, HiRes, TA, Veritas, Milagro (NSF-AST, DOE-HEP, Japan, Korea, Canada, Ireland, Smithsonian, 17 more countries) • Neutrinos: Borexino, Double Chooz, CUORE (DOE- NP, INFN, France, Germany, Brazil, Japan, Russia, Spain, UK) • Structure of the Universe: ACT, SPT (NSF-AST, OPP) • B-Mode Polarization of CMB: QUIET (NSF-AST) • Origin of the Elements: NSCL (DOE-NP) RecentRecent SourcesSources ofof CommunityCommunity InputInput Workshops NRC Physics 2010 Reports 7 LargeLarge HadronHadron ColliderCollider atat CERNCERN 27 km Tunnel in Switzerland & France /+&352-(&7 3= 3; 81'(5*5281':25.6 CMS3RLQW 30 3; 30 7; 8- 8- 8- 5$ 3 0 ([LVWLQJ 8; 5= 8;& 8- 8- ([LVWLQJ 5$ TOTEM 55 8/ 8- 8- 3; 55 8/ 8$ 3,//$5 8' 8/ 86 8/ 86 & 7' 30 3= 8$ 78 8: 8- ALICE 83 5$ 3= 8- 7; 5= &06 8- 3RLQW 8$ 8; 8- 8/ 8- 8- 8- 3RLQW 5$ 8/ 30 8: 86 8$ 8- 8- 7' 7= 3RLQW 3RLQW 1 8' 83 3RLQW 8$ 30 3*& 8/ 3RLQW 5$ 30 ¾ 34 Agencies fund ATLAS 83 55 86 7= 8- 8: 8- 3; 8/ 3RLQW 8; 636 55 8$ 30 8- 77 8: 3; 8$ $/,&( 8- 8- 3RLQW 3*& 3= 5$ /66 3RLQW 30 8/ 5+ 86 ¾ 31 Agencies fund CMS 3; 30 3; 7= 7- 8- 30, 3; 8$ 8/ 5$ 8- 8- 86 7, 8- 55 8/ 8/ 8- 8- 7, 7; ([LVWLQJ6WUXFWXUHV 8- 55 8- 57 8- 5$ /+&3URMHFW6WUXFWXUHV 5+ 8; 7, 8- 8- 8; 7, /+&([FDYDWHG6WUXFWXUHV 57 ¾ Billion-dollar detectors 86$ /+&¶%· 67&(OMU /+&&RPSOHWHG6WUXFWXUHV &( $7/$6 LHCb /+&&RPSOHWHG6WUXFWXUHV &9(/+00$ ATLAS 8 DeepDeep UndergroundUnderground ScienceScience andand EngineeringEngineering LaboratoryLaboratory (DUSEL)(DUSEL) • DUSEL is being envisioned as a unique, dedicated international underground education & research facility that would support potentially transformational experiments in multiple disciplines. • The U.S. particle, nuclear, and astrophysics communities have selected DUSEL as central to their national programs. • The engineering, geology and biology communities are proactively engaged, and participate in all aspects of DUSEL planning. • Development focused on the former Homestake Gold Mine (Lead, SD), the deepest mine in North America. Davis Cavern Sep 21, 2009 9 P5 NSF NSAC Review LRP NSF P5NSF Review Review NSF Annual Review S4 Awards PDR PASAG NSB Approves PDR 10 HomestakeHomestake –– HomeHome toto thethe DavisDavis DetectorDetector (Nobel(Nobel Prize,Prize, Physics,Physics, 2002)2002) Raymond Davis, Jr. Ray Davis 1965 Raymond Davis, Jr. was awarded the 2002 Nobel Prize in Physics "for pioneering contributions to astrophysics, in particular for the detection of cosmic neutrinos." He was the first scientist to detect solar neutrinos, ghostlike particles produced in the nuclear reactions that power the sun. In research from 1967– 1985 conducted at the Homestake Gold Mine, he consistently found only one‐third of the neutrinos that standard theories predicted. Experiments in the Davis Cavern 1990s using different detectors around the world eventually confirmed the solar neutrino discrepancy. Sep 21, 200911 Aerial View of Homestake Site Water Treatment Plant Open Yates Complex Cut Town of Lead SDSTA 1km Surface Rights Kirk Ross Complex Canyon Access 12 CurrentlyCurrently EnvisionedEnvisioned DUSELDUSEL LaboratoryLaboratory FootprintFootprint Yates Shaft Ross Shaft 300’ Campus Davis Cavity 4850’ Lab Modules Large Cavity 4850’ Campus New Winze Lab Module at 7400 7400’ Campus Deep Drilling Facility at 7400’ #6 Winze 13 DUSELDUSEL SolicitationSolicitation ProcessProcess • Initiated at Town Meeting at NSF, March 2004. • Solicitation 1 (S1): – Define site‐independent science scope and infrastructure needs; unify the community (awarded Jan 2005). • Solicitation 2 (S2): – Develop conceptual designs (8 received, 2 awarded, Sep 2005). • Solicitation 3 (S3): – Site selection to initiate facility design for 1 potential MREFC candidate (4 received, 1 awarded –Homestake, U.C. Berkeley). – Total facility design: $47M from FY 2007 through FY 2011. • Solicitation 4 (S4): – Initiate technical designs for candidates for the DUSEL suite of experiments. – 25 proposals received January 9, 2009; reviewed spring 2009. – $21M total over three years, beginning in FY09. 14 DesignDesign ofof DUSELDUSEL FacilityFacility && InfrastructureInfrastructure • First NSF annual review of the DUSEL Design Project held at U.C. Berkeley in January 2009. – 25‐member multi‐disciplinary expert panel. • Recommended a proposal be submitted to NSF by UCB for funds to complete Preliminary Design. • Proposal submitted May 2009, reviewed by NSF. • Panel recommended to the NSF that proposal “must be funded.” • Put forward for consideration by the National Science Board in August and September 2009. 15 DevelopingDeveloping thethe DUSELDUSEL ExperimentalExperimental Program:Program: S4S4 • Solicitation 4 (S4): called for proposals to develop designs and pursue targeted R&D for potential candidates for the DUSEL suite of experiments. • 25 proposals received; 300 senior researchers named; 91 institutions. • Nine proposals funded in physics. • Seven proposals funded in BIO, – Dark matter GEO & ENG sciences: – Neutrino‐less double‐beta decay – Fracture processes – Large water Cerenkov detector (multipurpose) – Coupled processes – Underground accelerator – Subsurface imaging and sensing – Assaying sub‐facility – Fiber optic strain monitoring – CO sequestration • Total physics awards: $21M over 3 years. 2 – Eco‐hydrology & deep drilling • Total BGE awards: $3M. NSF is committed to a rich, diverse, and multi‐disciplinary DUSEL research program. 16 DUSELDUSEL TargetTarget TimelineTimeline forfor MREFCMREFC • January ’09: NSF Project Review #1. • February ’10: NSF Project Review #2. • December ’10: NSF Preliminary Design Review (PDR). • Spring ’11: Presentation of DUSEL MREFC proposal to National Science Board. Above targets an FY 2013 construction start. 17 NSF/DOENSF/DOE CollaborationCollaboration • NSF/DOE agreed to establish DUSEL Physics Joint Oversight Group (JOG) immediately after release of P5 report (May ’08). – NSF/PHY, DOE/OHEP, DOE/ONP. – Builds on successful NSF & DOE collaboration on Large Hadron Collider (LHC) in high energy physics. • DUSEL JOG will coordinate & oversee DUSEL experimental physics program. • DUSEL JOG Joint Statement of Intent transmitted to OMB/OSTP by NSF Director and DOE Under Secretary for Science (Aug ’09). – MoU in approximately 1 year. – Close coordination of evolving design. – Joint review process. 18 19 SouthSouth DakotaDakota DevelopmentDevelopment ofof SanfordSanford LabLab • South Dakota Science and Technology Authority (SDSTA) holds $124M for development of Sanford Laboratory. – $70M private
Load more

Recommended publications
  • Realization of the Low Background Neutrino Detector Double Chooz: from the Development of a High-Purity Liquid & Gas Handling Concept to first Neutrino Data
    Realization of the low background neutrino detector Double Chooz: From the development of a high-purity liquid & gas handling concept to first neutrino data Dissertation of Patrick Pfahler TECHNISCHE UNIVERSITAT¨ MUNCHEN¨ Physik Department Lehrstuhl f¨urexperimentelle Astroteilchenphysik / E15 Univ.-Prof. Dr. Lothar Oberauer Realization of the low background neutrino detector Double Chooz: From the development of high-purity liquid- & gas handling concept to first neutrino data Dipl. Phys. (Univ.) Patrick Pfahler Vollst¨andigerAbdruck der von der Fakult¨atf¨urPhysik der Technischen Universit¨atM¨unchen zur Erlangung des akademischen Grades eines Doktors des Naturwissenschaften (Dr. rer. nat) genehmigten Dissertation. Vorsitzender: Univ.-Prof. Dr. Alejandro Ibarra Pr¨uferder Dissertation: 1. Univ.-Prof. Dr. Lothar Oberauer 2. Priv.-Doz. Dr. Andreas Ulrich Die Dissertation wurde am 3.12.2012 bei der Technischen Universit¨atM¨unchen eingereicht und durch die Fakult¨atf¨urPhysik am 17.12.2012 angenommen. 2 Contents Contents i Introduction 1 I The Neutrino Disappearance Experiment Double Chooz 5 1 Neutrino Oscillation and Flavor Mixing 6 1.1 PMNS Matrix . 6 1.2 Flavor Mixing and Neutrino Oscillations . 7 1.2.1 Survival Probability of Reactor Neutrinos . 9 1.2.2 Neutrino Masses and Mass Hierarchy . 12 2 Reactor Neutrinos 14 2.1 Neutrino Production in Nuclear Power Cores . 14 2.2 Energy Spectrum of Reactor neutrinos . 15 2.3 Neutrino Flux Approximation . 16 3 The Double Chooz Experiment 19 3.1 The Double Chooz Collaboration . 19 3.2 Experimental Site: Commercial Nuclear Power Plant in Chooz . 20 3.3 Physics Program and Experimental Concept . 21 3.4 Signal . 23 3.4.1 The Inverse Beta Decay (IBD) .
    [Show full text]
  • Results in Neutrino Oscillations from Super-Kamiokande I
    Status of the RENO Reactor Neutrino Experiment RENO = Reactor Experiment for Neutrino Oscillation (For RENO Collaboration) K.K. Joo Chonnam National University February 15, 2011 Research Techniques Seminar @FNAL Outline Experiment Goals of the RENO Exp. - Short introduction - Expected q13 sensitivity - Systematic uncertainty Overview of the RENO Experiment - Experimental Setup of RENO - Schedule - Tunnel excavation - Status of detector construction - DAQ, data analysis tools Summary Brief History of Neutrinos 1930: Pauli postulated neutrino to explain b decay problem 1933: Fermi baptized the neutrino in his weak-interaction theory 1956: First discovery of neutrino by Reines & Cowan from reactor 1957: Neutrinos are left-handed by Glodhaber et al. 1962: Discovery of nm by Lederman et al. (Brookhaven Lab) 1974: Discovery of neutral currents due to neutrinos 1977: Tau lepton discovery by Perl et al. (SLAC) 1998: Atmospheric neutrino oscillation observed by Super-K 2000: nt discovery by DONUT (Fermilab) 2002: Solar neutrino oscillation observed by SNO and confirmed by Kamland What NEXT? Standard Model Neutrinos in SM Neutrino Oscillation . Three types of neutrinos exist & mixing among them Oscillation parameters (q12 , q23 , q13) Not measured yet . Elementary particles with almost no interactions . Almost massless: impossible to measure its mass Neutrino Mixing Parameters Matrix Components: νe Ue1 Ue2 Ue3 ν1 3 Angles (θ ; θ ; θ ) 12 13 23 ν U U U ν 1 CP phase (δ) μ μ1 μ2 μ3 2 2 Mass differences ντ Uτ1 Uτ2 Uτ3 ν3 1 0 0 c 0 s ei c s 0 13 13 12 12 U 0 c23 s23 0 1 0 s12 c12 0 i 0 s23 c23 s13e 0 c13 0 0 1 atmospheric SK, K2K The Next Big Thing? SNO, solar SK, KamLAND ≈ ≈ ° q23 qatm 45 q12 ≈qsol ≈ 32° Large and maximal mixing! Reduction of reactor neutrinos due to oscillations Disappearance Reactor neutrino disappearance Prob.
    [Show full text]
  • Letter of Interest Forthcoming Science from The
    Snowmass2021 - Letter of Interest Forthcoming Science from the PROSPECT-I Data Set Neutrino Frontier Topical Groups: (NF02) Sterile neutrinos (NF03) Beyond the Standard Model (NF07) Applications (NF09) Artificial neutrino sources Contact Information: Nathaniel Bowden (LLNL) [[email protected]] Karsten Heeger (Yale University) [[email protected]] Pieter Mumm (NIST) [[email protected]] M. Andriamirado,6 A. B. Balantekin,16 H. R. Band,17 C. D. Bass,8 D. E. Bergeron,10 D. Berish,13 N. S. Bowden,7 J. P.Brodsky,7 C. D. Bryan,11 R. Carr,9 T. Classen,7 A. J. Conant,4 G. Deichert,11 M. V.Diwan,2 M. J. Dolinski,3 A. Erickson,4 B. T. Foust,17 J. K. Gaison,17 A. Galindo-Uribarri,12, 14 C. E. Gilbert,12, 14 C. Grant,1 B. T. Hackett,12, 14 S. Hans,2 A. B. Hansell,13 K. M. Heeger,17 D. E. Jaffe,2 X. Ji,2 D. C. Jones,13 O. Kyzylova,3 C. E. Lane,3 T. J. Langford,17 J. LaRosa,10 B. R. Littlejohn,6 X. Lu,12, 14 J. Maricic,5 M. P.Mendenhall,7 A. M. Meyer,5 R. Milincic,5 I. Mitchell,5 P.E. Mueller,12 H. P.Mumm,10 J. Napolitano,13 C. Nave,3 R. Neilson,3 J. A. Nikkel,17 D. Norcini,17 S. Nour,10 J. L. Palomino,6 D. A. Pushin,15 X. Qian,2 E. Romero-Romero,12, 14 R. Rosero,2 P.T. Surukuchi,17 M. A. Tyra,10 R. L. Varner,12 D. Venegas-Vargas,12, 14 P.B.
    [Show full text]
  • APC Scientific Board 2017 Tech
    2012-2016 APC Laboratory Technical Activities T. Zerguerras on behalf of the Technical Departments 20/11/2017 APC Scientific Board 2017 1 Technical Departments Organisation Equipment, facilities and platform Instrumentation Department (Techniques Expérimentales) Electronics and Microelectronics Department Mechanics Department IT Department Quality Unit R&D: CMB µelectronic, Compton, GAMMACUBE, Liquido Analysis & Prospects 20/11/2017 APC Scientific Board 2017 2 General organisation • 5 technical departments + Quality Unit + the FACe platform • Building an instrument => combining skills 22/09/2017 APC Scientific Board 2017 3 Technical departments organisation Matrix organisation structure: Project/Department (Assignment to a department, participation to projects) One specific skill (Mechanics, Electronics/µelectronics, Instrumentation, IT, QA/PA) Transverse activities of the Quality Unit Supervision : Head of department Project coordination: Project manager Indicator Boards for activities and assignments monitoring Project Monitoring Committee (Comité de Suivi de Projets CSP) This organisation aims to create a bond of trust with funding and tutelage agencies 20/11/2017 APC Scientific Board 2017 4 Organisation: Technical staff evolution On 31/12 Technical departments staff evolution 60 Technical departments staff - Gender 45 50 40 40 35 34 30 30 33 35 38 38 Permanent 25 MEN Fixed-term 20 38 40 39 40 39 20 WOMEN 15 10 10 15 17 13 12 12 5 10 11 9 10 11 0 0 2012 2013 2014 2015 2016 2012 2013 2014 2015 2016 Technical departments
    [Show full text]
  • Muon Spallation in Double Chooz
    Muon Spallation in Double Chooz Claire Thomas∗ REU, Columbia University and MIT (Dated: August 10, 2009) This report presents my work for Double Chooz at MIT during the 2009 Summer REU program, funded by Columbia University. Double Chooz is a reactor neutrino experiment that aims to measure the mixing parameter θ13. The experiment detects electron antineutrinos via inverse beta decay. Neutrons and light nuclei made in muon spallation are a major background to the experiment. The delayed neutron emitter 9Li is especially problematic because it mimics the inverse beta decay signal. For this reason I studied muon spallation in Double Chooz, focusing on the production and subsequent decay of 9Li. There are two key differences between 9Li decay and inverse beta decay. The first is that 9Li is a β− decay, so it emits an electron, whereas inverse beta decay emits a positron. The second difference is the energy of the neutrons emitted. In 9Li decay the neutron energy is on the order of MeV, whereas the inverse beta decay neutron has a negligible kinetic energy. Since Double Chooz does not distinguish charge, the positrons and electrons are not easy to distinguish. First, I ran simulations of electrons and positrons in the Double Chooz detector and constructed a late light variable to distinguish them from electrons. This proved insufficient, so I wrote general software to simulate radioactive decays in the Double Chooz detector. In this report I present the deposited energy spectra of a few important decays. 1. INTRODUCTION The consequence of neutrino oscillation is that an ex- periment that is sensitive to only one of the three neu- 1.1.
    [Show full text]
  • Neutrino Oscillation Studies with Reactors
    REVIEW Received 3 Nov 2014 | Accepted 17 Mar 2015 | Published 27 Apr 2015 DOI: 10.1038/ncomms7935 OPEN Neutrino oscillation studies with reactors P. Vogel1, L.J. Wen2 & C. Zhang3 Nuclear reactors are one of the most intense, pure, controllable, cost-effective and well- understood sources of neutrinos. Reactors have played a major role in the study of neutrino oscillations, a phenomenon that indicates that neutrinos have mass and that neutrino flavours are quantum mechanical mixtures. Over the past several decades, reactors were used in the discovery of neutrinos, were crucial in solving the solar neutrino puzzle, and allowed the determination of the smallest mixing angle y13. In the near future, reactors will help to determine the neutrino mass hierarchy and to solve the puzzling issue of sterile neutrinos. eutrinos, the products of radioactive decay among other things, are somewhat enigmatic, since they can travel enormous distances through matter without interacting even once. NUnderstanding their properties in detail is fundamentally important. Notwithstanding that they are so very difficult to observe, great progress in this field has been achieved in recent decades. The study of neutrinos is opening a path for the generalization of the so-called Standard Model that explains most of what we know about elementary particles and their interactions, but in the view of most physicists is incomplete. The Standard Model of electroweak interactions, developed in late 1960s, incorporates À À neutrinos (ne, nm, nt) as left-handed partners of the three families of charged leptons (e , m , t À ). Since weak interactions are the only way neutrinos interact with anything, the un-needed right-handed components of the neutrino field are absent in the Model by definition and neutrinos are assumed to be massless, with the individual lepton number (that is, the number of leptons of a given flavour or family) being strictly conserved.
    [Show full text]
  • PROSPECT Upgrade
    Precision Reactor Upgrade significantly expands oscillation Oscillation and physics reach in unique parameter space ] prospect.yale.edu ] ] 2 2 90% CL 90% CL 2 90% CL SPECTrum Experiment: PROSPECT, 1 yr Sensitivity PROSPECT, 2 yr Optimized Sensitivity PROSPECT, 2 yr Optimized Sensitivity PROSPECT, 2 yr Sensitivity DANSS Exclusion PROSPECT, 2 yr Optimized Sensitivity, σspectrum = 5% [eV [eV PROSPECT, 2 yr Optimized Sensitivity NEOS Exclusion [eV DYB Exclusion KATRIN Exclusion 2 41 PROSPECT, Current Sensitivity 2 41 STEREO, Current Exclusion 2 41 PROSPECT-I demonstrated PROSPECT, Current Exclusion STEREO, Expected Sensitivity LBN CPV Ambiguity Limit m m 10 m SBL + Gallium Anomaly (RAA + Evolution), 95% CL Δ 10 Δ 10 Upgrade & Science Goals Δ excellent performance H. Pieter Mumm for the PROSPECT collaboration 6 Primary Physics Goals Li capture Search for sterile neutrino oscillation 1 1 1 • Nuclear recoil within unique parameter space important for the reactor anomaly and Long Baseline Electronic recoil experiments. 235 • High-resolution U spectrum and flux 10−1 10−1 10−1 measurement addresses observed shape 10−2 10−1 1 10−2 10−1 1 10−2 10−1 1 sin22θ sin22θ sin22 discrepancies 14 14 θ14 Pulse shape discrimination (PSD) PROSPECT measurement strategy capable scintillator with high light yield • Unique 6Li-doped liquid scintillator as inverse Left: Comparison of sterile oscillation sensitivities for current and projected PROSPECT-II datasets. allows for excellent background beta decay target; distinct IBD topology Center: Projected PROSPECT-II sensitivity compared to selected short-baseline reactor experiments. rejection and > 5%/ E resolution. • Highly segmented array for background Right: Overlap of three year PROSPECT-II sensitivity with relevant regions of parameter space rejection and event localization • ~ 7m baseline to very compact highly- PROSPECT-II uniquely addresses a high Δ m2 region between enriched reactor core provides unique 1 eV2 - 15 eV2, and will reach the 5o sin2(2�14) sensitivity over sensitivity at high Δ m2.
    [Show full text]
  • Double Chooz: the Show Goes On!
    Double Chooz: The Show Goes On! Lindley Winslow University of California Los Angeles On behalf of the Double Chooz Collaboration The Double Chooz Collaboration: Brazil France Germany Japan Russia Spain USA CBPF APC EKU Tübingen Tohoku U. INR RAS CIEMAT- U. Alabama UNICAMP CEA/DSM/ MPIK Tokyo Inst. Tech. IPC RAS Madrid ANL UFABC IRFU: Heidelberg Tokyo Metro. U. RRC U. Chicago SPP RWTH Aachen Niigata U. Kurchatov Columbia U. SPhN TU München Kobe U. UCDavis SEDI U. Hamburg Tohoku Gakuin U. Drexel U. SIS Hiroshima Inst. IIT SENAC Tech. KSU CNRS/IN2P3: LLNL Subatech MIT IPHC U. Notre Dame Spokesperson: U. H. de Kerret (IN2P3) Tennessee Project Manager: Ch. Veyssière (CEA-Saclay) Web Site: www.doublechooz.org/ 2 Theory favored small sin 2θ13! Model Review Theory Order of Magnitude Prediction by Albright et. al. ArXiv:0803.4176 Le-Lμ-Lτ 0.00001 SO(3) 0.00001 Neutrino Factory S3 and S4 0.001 Designs A4 Tetrahedral 0.001 Texture Zero 0.001 Reactor Experiment RH Dominance 0.01 Design SO(10) with Sym/Antisym 0.01 Contributions Limit as SO(10) with lopsided 0.1 masses of 2011 Measuring the last mixing angle: 1.0 Probability 2 2 2 P = 1 - sin 2!13 sin (1.27 "m L/E)! Distance ~1000 meters Measuring the last mixing angle: 1.0 Probability 2 2 2 P = 1 - sin 2!13 sin (1.27 "m L/E)! Distance ~1000 meters Remember: We are looking for an effect as a function of L/E. Construction Underway! Double Chooz Analysis is Unique: • Analysis uses BOTH Rate and Energy information ➙Detailed Energy Response Model • Simple Reactor Configuration ➙ Multiple analysis periods.
    [Show full text]
  • Highlight Talk from Super-Kamiokande †
    Communication Highlight Talk from Super-Kamiokande † Yuuki Nakano and on behalf of the Super-Kamiokande Collaboration Kamioka Observatory, Institute for Cosmic Ray Research, The University of Tokyo, Higashi-Mozumi 456, Kamioka-cho, Hida-city Gifu 506-1205, Japan; [email protected]; Tel.: +81-578-85-9665 † This paper is based on the talk at the 7th International Conference on New Frontiers in Physics (ICNFP 2018), Crete, Greece, 4–12 July 2018. Received: 30 November 2018; Accepted: 7 January 2019; Published: 9 January 2019 Abstract: Super-Kamiokande (SK), a 50 kton water Cherenkov detector in Japan, is observing both atmospheric and solar neutrinos. It is also searching for supernova (relic) neutrinos, proton decays and dark matter-like particles. A three-flavor oscillation analysis was conducted with the atmospheric neutrino data to study the mass hierarchy, the leptonic CP violation term, and other oscillation parameters. In addition, the observation of solar neutrinos gives precise measurements of the energy spectrum and oscillation parameters. In this proceedings, we given an overview of the latest results from SK and the prospect toward the future project of SK-Gd. Keywords: Super-Kamiokande; atmospheric neutrino; solar neutrino; neutrino oscillation; CP violation; proton decay 1. Introduction A theoretical framework of neutrino oscillation has been established in the past 50 years [1,2]. Neutrino physics has been dominated by the measurement of oscillation parameters and such measurements suggest that neutrinos are massive and mixing in the lepton sector [3]. Within the three- 2 2 flavor framework, three mixing angles (q12, q23, and q13) and two mass splittings (Dm21 and Dm32,31) are measured among neutrino experiments.
    [Show full text]
  • Overview of Hyper-Kamiokande
    Overview of Hyper-Kamiokande Masato Shiozawa ANT11 Workshop, Oct.-10-2011 Kamioka Observatory, Institute for Cosmic Ray Research, U of Tokyo, and Kamioka Satellite, Institute for the Mathematics and Physics of the Universe, U of Tokyo Establish θ13, then CP violation T2K collaboration, PRL107,041801(2011) Fogli et al., arXiv1106.6028 T2K observed indication of νμ→νe titled “Evidence of θ13>0 from global ν analysis” Data ν Osc. e CC ν ν MeV) μ+ μ CC 3 ν e CC NC 2 Nobs : 6 νe candidates Nexp : 1.5±0.3(syst) 2 for sin 2θ13=0 1 nonzero θ13 at 2.5σ Number of events /(250 Number of events 0 0 1000 2000 3000 ν Reconstructed energy (MeV) nonzero θ13 is already >3σ w/ solar and reactorν ‣T2K aims to establish nonzero θ13 and measure it w/ more data ‣reactor experiments are starting data taking (Double CHOOZ, RENO, Daya Bay) It’s now time to seriously think about next generation 2 experiments assuming θ13≠0 (sin θ13= a few %). Hyper-K WG, arXiv:1109.3262 [hep-ex] Letter of Intent: The Hyper-Kamiokande Experiment — Detector Design and Physics Potential — K. Abe,12, 14 T. Abe,10 H. Aihara,10, 14 Y. Fukuda,5 Y. Hayato,12, 14 K. Huang,4 A. K. Ichikawa,4 M. Ikeda,4 K. Inoue,8, 14 H. Ishino,7 Y. Itow,6 T. Kajita,13, 14 J. Kameda,12, 14 Y. Kishimoto,12, 14 M. Koga,8, 14 Y. Koshio,12, 14 K. P. Lee,13 A. Minamino,4 M. Miura,12, 14 S.
    [Show full text]
  • APC - Astroparticule Et Cosmologie Rapport Hcéres
    APC - Astroparticule et cosmologie Rapport Hcéres To cite this version: Rapport d’évaluation d’une entité de recherche. APC - Astroparticule et cosmologie. 2013, Université Paris Diderot - Paris 7, Commissariat à l’énergie atomique et aux énergies alternatives - CEA, Centre national de la recherche scientifique - CNRS, L’Observatoire de Paris. hceres-02031598 HAL Id: hceres-02031598 https://hal-hceres.archives-ouvertes.fr/hceres-02031598 Submitted on 20 Feb 2019 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Department for the evaluation of research units AERES report on unit: AstroParticule et Cosmologie APC Under the supervision of the following institutions and research bodies: Université Paris 7 - Denis Diderot Centre National de la Recherche Scientifique Commissariat à l’Energie Atomique et aux Energies Alternatives Observatoire de Paris January 2013 Research Units Department The president of AERES "signs[...], the evaluation reports, [...]countersigned for each evaluation department by the relevant head of department (Article 9, paragraph 3, of french decree n°2006-1334 dated 3 november 2006, revised). Astro-Particule et Cosmologie, APC, UP7, CNRS, CEA, Observatoire de Paris, Mr Pierre BINETRUY Grading Once the visits for the 2012-2013 evaluation campaign had been completed, the chairpersons of the expert committees, who met per disciplinary group, proceeded to attribute a score to the research units in their group (and, when necessary, for these units’ in-house teams).
    [Show full text]
  • The Double Chooz Experiment
    The Double Chooz experiment M. Goger-Neff,¨ M. Franke, N. Haag, M. Hofmann, L. Oberauer, P. Pfahler, W. Potzel, S. Schonert,¨ H. TrinhThi, V. Zimmer Introduction The goal of the Double Chooz experiment is the precise determination of the neutrino mixing angle θ13. Two iden- tical detectors measure the electron antineutrinos emitted from two nuclear reactors at the Chooz nuclear power sta- tion in France. The far detector in 1 km distance from the reactor cores started data taking in April 2011. A second near detector at a distance of about 400 m from the reactors is currently under construction and will start data taking in 2014. The near detector will monitor the unoscillated neu- trino flux whereas the far detector is searching for a disap- pearance effect due to neutrino oscillations. If the electron antineutrinos change their flavor (for a nonzero value of θ13), a reduced electron antineutrino flux is observed at the far detector. Detector Setup The target of the Double Chooz detector consists of about 8 tons of a newly developed Gadolinium-loaded liq- uid scintillator. The detection reaction is the inverse beta + decay: ν¯e + p ! n + e . The positron created in this re- action provides a prompt scintillation light signal and car- ries the energy information of the neutrino. The neutron is captured with high probability on the Gd dissolved in Figure 1: Setup of the Double Chooz detectors. the target scintillator with a typical delay time of ∼ 30µs releasing gamma radiation with a total energy of about 8 MeV. This coincidence allows an efficient neutrino de- tection and background reduction.
    [Show full text]